Microturbulence , macroturbulence , thermal motion , and rotation contribute to the broadening of line profiles in stellar spectra . Reliable data on the velocity distribution of turbulent motions in stellar atmospheres are needed to interpret the spectra of solar-type stars unambiguously in exoplanetary research . Stellar spectra with a high resolution of 115000 obtained with the HARPS spectrograph provide an opportunity to examine turbulence velocities and their depth distributions in the photosphere of stars . Fourier analysis was performed for 17 iron lines in the spectra of 13 stars with an effective temperature of 4900–6200 K and a logarithm of surface gravity of 3.9–5.0 as well as in the spectrum of the Sun as a star . Models of stellar atmospheres were taken from the MARCS database . The standard concept of isotropic Gaussian microturbulence was assumed in this study . A satisfactory fit between the synthesized profiles of spectral lines and observational data verified the reliability of the Fourier method . The most likely estimates of turbulence velocities , the rotation velocity , and the iron abundance and their photospheric depth distribution profiles were obtained as a result . Microturbulence does not vary to any significant degree with depth , while macroturbulence has a marked depth dependence . The macroturbulence velocity increases with depth in the stellar atmosphere . The higher the effective temperature of a star and the stronger the surface gravity , the steeper the expected macroturbulence gradient . The mean macroturbulence velocity increases for stars with higher temperatures , weaker gravity , and faster rotation . The mean macro- and microturbulence velocities are correlated with each other and with the rotation velocity in the examined stars . The ratio between the macroturbulence velocity and the rotation velocity in solar-type stars varies from 1 ( the hottest stars ) to 1.7 ( the coolest stars ) . The age dependence of the rotation velocity is more pronounced than that of the velocity of macroturbulent motions .